[1]} computed \(\varepsilon _r= \log _{10} (-\Delta \ln e/ f)\)  for each binary in their sample. When these authors plotted the orbital eccentricities of their binaries as a function of \(\varepsilon _r\) , they found that the value \(\varepsilon _{\mathrm {crit}}= \log _{10} (3)\)  was a relevant boundary between circularized and non-circularized systems. Thus, they confirmed the results that [2]} obtained on a smaller sample. In addition, [1]} demonstrated that the dissipation of tidal inertial waves in the deep convective envelopes of RG can be neglected [4]}, [5]}, [6]} because these stars are close to the configuration of a full convective sphere where this mechanism becomes less efficient [7]}. They also showed that this \(\varepsilon _{\mathrm {crit}}\)  marked the separating line between oscillating and non-oscillating systems, indicating that the non-oscillating binaries are those with short circularization timescales.
